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The nature of the late B-type stars HD 67044 and HD42035

R. Monier12 • M. Gebran3• F. Royer4

Abstract While monitoring a sample of apparentlyslowly rotating superficially normal bright late B andearly A stars in the northern hemisphere, we have dis-covered that HD 67044 and HD 42035, hitherto clas-sified as normal late B-type stars, are actually respec-tively a new chemically peculiar star and a new spectro-scopic binary containing a very slow rotator HD 42035 Swith ultra-sharp lines (ve sin i = 3.7 km s−1) and a fastrotator HD 42035 B with broad lines. The lines of Ti II,Cr II, Mn II, Sr II , Y II, Zr II and Ba II are conspic-uous features in the high resolution SOPHIE spectrum(R = 75000) of HD 67044. The Hg II line at 3983.93 Ais also present as a weak feature. The composite spec-trum of HD 42035 is characterised by very sharp linesformed in HD 42035 S superimposed onto the shallowand broad lines of HD 42035 B. These very sharp linesare mostly due to light elements from C to Ni, the onlyheavy species definitely present are strontium and bar-ium. Selected lines of 21 chemical elements from He upto Hg have been synthesized using model atmospherescomputed with ATLAS9 and the spectrum synthesiscode SYNSPEC48 including hyperfine structure of var-ious isotopes when relevant. These synthetic spectrahave been adjusted to high resolution high signal-to-noise spectra of HD 67044 and HD 42035 S in order toderive abundances of these key elements. HD 67044 isfound to have distinct enhancements of Ti, Cr, Mn, Sr,

R. Monier

LESIA, UMR 8109, Observatoire de Paris, place J. Janssen,Meudon.

Laboratoire Lagange, Universite de Nice Sophia, Parc Valrose,06100 Nice, France.

M. Gebran

Department of Physics and Astronomy, Notre Dame University-Louaize, PO Box 72, Zouk Mikael, Lebanon.

F. Royer

GEPI, Observatoire de Paris, place J. Janssen, Meudon, France.

Y, Zr, Ba and Hg and underabundances in He, C, O, Ca

and Sc which shows that this star is not a superficially

normal late B-type star, but actually is a new CP starmost likely of the HgMn type. HD 42035 S has provi-

sional underabundances of the light elements from C to

Ti and overabundances of heavier elements (except for

Fe and Sr which are also underabundant) up to barium.These values are lower limits to the actual abundances

as we cannot currently place properly the continuum

of HD 42035 S. More accurate fundamental parameters

and abundances for HD 42035 S and HD 42035 B willbe derived if we manage to disentangle their spectra.

They will help clarify the status of the two components

in this interesting new spectroscopic binary.

Keywords stars: early-type – stars: abundances –

stars: chemically peculiar - stars: spectroscopic binary

1 Introduction

We have recently undertaken a spectroscopic survey of

all apparently slowly rotating bright early A stars (A0-

A1V) and late B stars (B8-B9V) observable from thenorthern hemisphere. The incentive is to search for

rapid rotators seen pole-on or new chemically pecu-

liar B and A stars which have thus far remained un-

noticed. This project addresses fundamental questions

of the physics of late-B and early-A stars: i) can wefind new instances of rapid rotators seen pole-on (other

than Vega) and study their physical properties (gra-

dient of temperature across the disk, limb and grav-

ity darkening), ii) is our census of Chemically Peculiarstars complete up to the magnitude limits we adopted

? If not, what are the physical properties of the newly

found CP stars?. The abundance results for the A0-

A1V sample have been published in Royer et al. (2014).The selection criteria were: a declination higher than

2

−15◦, spectral class A0 or A1 and luminosity class V

and IV and magnitudes V brighter than 6.65 and ave sin iless than 65 km s−1. The B8-9 sample employs

the same criteria, except for the V magnitude brighter

than 7.85 as these B stars are intrinsically brighter in

the V band where SOPHIE reaches its maximum ef-ficiency. Most of the stars of that B8-9 sample (40

stars) have been observed in December 2014 with SO-

PHIE, the echelle high-resolution spectrograph at Ob-

servatoire de Haute Provence yielding spectra coving

the 3900 A-6800 A spectral ranger over 39 orders at aresolving power R = 75000. A careful abundance analy-

sis of the high resolution high signal-to-noise ratio spec-

tra of the A stars sample has allowed to sort out the

sample of 47 A stars into 17 chemically normal stars (ie.whose abundances do not depart by more than ±0.20

dex from solar values), 12 spectroscopic binaries and

13 chemically peculiar stars (CPs) among which five

are new CP stars. The status of these new CP stars

still needs to be fully specified by spectropolarimetricobservations to address their magnetic nature or by ex-

ploring new spectral ranges which we had not explored

in this first study. Indeed, the abundance analysis of

the A stars sample in Royer et al. (2014) relied only onfour spectral regions: 4150–4300A, 4400–4790A, 4920–

5850 A, and 6000–6275A, avoiding Balmer lines and at-

mospheric telluric lines.

We have now started to examine the B9-B8V sample us-

ing the full wavelength coverage provided by SOPHIEto search for new Chemically Peculiar stars. We have

already reported on the discovery of 4 new HgMn stars

(Monier et al. 2015) whose spectra display strong Hg II

lines at 3984 A and strong Mn II lines. These newHgMn stars are HD 18104, HD 30085, HD 32867, HD

53588. In the process of our analysis of the B9-B8V

sample, we have just found that HD 67044, currently

classified B8 in SIMBAD, is actually another new CP

star, most likely another new HgMn star and that HD42035, classified B9V, actually is a new spectroscopic

binary containing a slow rotator which we will refer to

as HD 42035 S (S for ”sharp” lines) and a fast rota-

tor, HD 42035 B (B for ”broad” lines). A bibliographicquery of the CDS for HD 67044 and HD 42035 actually

reveals only 4 and 26 publications respectively. Neither

HD 67044 nor HD 42035 appear in Cowley’s classifica-

tion (1972) of the bright B8 stars. The purpose of this

paper is to report on the detection of strong Ti II, Cr II,Mn II, Sr II, Y II, Zr II, Ba II lines and a weak Hg II

line in the spectrum of HD 67044 and perform a line

identification of all the very sharp lines of HD 42035 S.

We also have determined the abundances of 17 chem-ical elements for HD 67044 using spectrum synthesis

to quantify the enhancements and depletions of these

elements. As several of the lines of HD 42035 S are

blended with those of HD 42035 B, we have only beenable to derive provisional abundances for HD 42035 S

using lines little affected by the fast rotator.

2 Observations and reduction

HD 67044 and HD 42035 have been observed at Ob-

servatoire de Haute Provence using the high resolution

(R = 75000) mode of the SOPHIE echelle spectrograph(Perruchot et al. 2008) in December 2014. The S

Nra-

tio of the spectra are about 130 and 174 at 5500 A

respectively. The observations log is displayed in Ta-

ble 1. The data are automatically reduced to produce1D extracted and wavelength calibrated echelle orders.

Each reduced order was normalised separately using a

Chebychev polynomial fit with sigma clipping, reject-

ing points above or below 1 σ of the local continuum.

Normalized orders were merged together, corrected bythe blaze function and resampled into a constant wave-

length step of about 0.02 A (see Royer et al. 2014, for

more details).

The radial velocities of HD 67044 and HD 42035 werederived from cross-correlation techniques, avoiding the

Balmer lines and the atmospheric telluric lines. The

normalized spectrum was cross-correlated with a syn-

thetic template extracted from the POLLUX database1

(Palacios et al. 2010) corresponding to the parametersTeff = 11000K, log g = 4 and solar abundances. A

parabolic fit of the upper part of the resulting cross-

correlation function yields the Doppler shift, which is

then used to shift spectra to rest wavelengths. The ra-dial velocities of HD 67044 and HD 42035 are collected

in Table 2.

3 The line spectrum of HD 67044

Several spectral regions have been used to establish the

chemical peculiarity of HD 67044. First, the red wing of

Hǫ, which lies in order 3, harbors the Hg II λ 3983.93 Aline and several Zr II and Y II lines likely to be strength-

ened in CP stars. After proper correction for the stellar

radial velocity, we found that HD 67044 does show the

Hg II 3983.93 A line as a feature absorbing about 2% ,

and also strong lines of Y II at 3982.59 A and of Zr II

at 3991.13 A and 3998.97 A. The Y II, Zr II and Hg II

lines in the spectral range 3980 to 4000 A are displayed

in figure 1 together with the synthetic spectrum fiting

best this spectral interval. Several other lines of Y II

1http://pollux.graal.univ-montp2.fr

3

and Zr II are strong absorbers in the spectrum of HD

67044 and have been used to derive the abundances inthese elements. Second, we examined the region from

4125 A to 4145 A (order 6) for the Si II lines at 4128.054

A and 4130.894 A and the Mn II line at 4136.92 A.

In an HgMn star, the Mn II line at 4136.92 A shouldbe strong whereas it should be absent in any compari-

son normal late B-type star. Furthermore, the lines of

Mn II at 4206.37 A and 4252.96 A should also be en-

hanced in the spectra of HgMn stars (Gray & Corbally

2009). These three Mn II lines correspond to mod-erately strong features in HD 67044, they usually are

broad lines absorbing 5% of the local continuum. Sev-

eral other strong Mn II lines could be found and have

been used to derive the abundance of manganese.We find that the strongest expected lines of Ti II,

Cr II, Mn II Sr II, Y II, Zr II, Ba II are all indeed

strong features in the spectrum of HD 67044. In Table

3, we give a list of the strongest unblended lines of these

species together with abundance determinations.The presence of the Hg II 3983.93 A line and of sev-

eral strong Mn II and Sr II, Y II and Zr II lines led us to

conclude that HD 67044 is actually another new HgMn

star and should be reclassified as such. The abundancedeterminations presented in next paragraph do confirm

this proposal.

3980 3985 3990 3995 4000Wavelength (A)

0.9

0.95

1

1.05

Nor

mal

ized

Flu

x

YII HgII ZrII ZrII

Fig. 1 Comparison of the observed Y II line at 3991.13A , Hg II at 3983.93 A and Zr II line at 3998.96 A of HD67044 to a synthetic profile computed for overabundancesof 1125 , 200 and 5000 times solar for yttrium, zirconiumand mercury respectively.

Table 1 Observation log

Star ID Spectral V Observation Exposure S/Ntype Date time (s )

HD 67044 B 8 7.48 2014-12-16 2400 130HD 42035 B9V 6.55 2014-12-18 750 174

4 The line spectrum of HD 42035

The high resolution spectrum of HD 42035 is charac-

terised by very sharp lines originating in HD 42035 S.

A first estimate of the projected equatorial rotational

velocity of HD 42035 S has been obtained by Fouriertransform analysis (Fig. 2), using the two Fe II lines

at 4508.29 and 4515.34 A. From the position of the

first zero of the Fourier transform, we derived a value

of ve sin i = 3.7 ± 0.2 km s−1. A close inspection of

the spectral region around the Mg II triplet at 4481A reveals that the spectrum of HD 42035 is actually

a composite spectrum containing shallow and broad

lines coming from HD 42035 B onto which are over-

imposed redshifted very sharp lines coming from HD42035 S. In the SOPHIE spectrum of HD 42035 ob-

tained in December 2014, the sharp lines of the Mg II

triplet are displaced, after correction for the barycen-

tric velocity of the Earth, by about +53.0 km s−1 with

respect to their laboratory positions. A comparison infigure 3 of our SOPHIE spectrum of HD 42035 with an

archival ELODIE spectrum (R=42000) obtained in De-

cember 2000 (also corrected for barycentric velocity of

the Earth) reveals large radial velocity variations of thesharp lines of the Mg II triplet and possibly a change

of the asymmetry of the broad and shallow Mg II line

formed in HD 42035 B. Indeed the shallow line had an

extended blue wing in December 2014 whereas it had

an extended red wing in December 2000. Recent spec-troscopy obtained at DAO by E. Griffin confirms large

radial velocity variations of the sharp lines and support

the binary nature of this star. The composite nature

of the spectrum is seen in many features, we show infigure 4 the region of Multiplet 7 of O I.

We have measured the centroids of all sharp lines

of HD 42035 S absorbing more than 2 % of the nor-

malized flux by adjusting gaussians. This yields wave-

lengths accurate to ±0.02 A. Seven hundred and thir-teen line centers were thus measured. In order to iden-

tify these lines, a model atmosphere was computed us-

ing ATLAS9 (Kurucz 1992) with 72 layers for the effec-

tive temperature and surface gravity of HD 42035 (seepar. 5.1) and a solar composition. A synthetic spec-

trum was then computed using SYNSPEC48 (Hubeny

& Lanz, 1992) over the entire range 3900 A to 6800

A for solar abundances and a microturbulent velocity

0.0 km s−1. It was further convolved with the ROTIN3routine (provided with SYNSPEC48) for the FWHM of

SOPHIE and the ve sin i of HD 42035 S. We found that

the following species are definitely present in HD 42035

S: He I, C I, C II, Mg II, N I, O I, Na I, Mg I, Mg II,Al I, Al II, Si I, Si II, S II, Ca I, Ca II, Sc I, Sc II, Ti II,

V II, Cr I, Cr II, Mn II, Fe I, Fe II, Co II, Sr II and Ba II

4

Fig. 2 Fourier transforms of the Fe II lines at 4508.29and 4515.34 A(solid lines) and of a synthetic profile with ave sin i = 3.7 kms−1 at a spectral resolution of 75000. Onthe velocity displayed on the x-axis, the position of the firstzero yields the projected equatorial rotational velocity.

4478 4480 4482 4484 4486Wavelength (A)

0.4

0.5

0.6

0.7

0.8

0.9

1

1.1

Nor

mal

ized

Flu

x

Fig. 3 Comparison of the composite Mg II triplet pro-file of HD 42035 taken 14 years apart: SOPHIE spectrum(solid line) and archival ELODIE spectrum (dashed line).The vertical lines depict the laboratory wavelengths of theMg II triplet.

(see Table 5). In contrast, the following elements have

very few lines identified and therefore their presence is

not confirmed: P II (only one line) and Nd II (only one

line). We note the absence of Y II lines and that of lines

of Hg II and Pt II characteristic of HgMn stars. Alsothe lines of Zr II are weak and we could only use one

6155 6156 6157 6158 6159 6160 6161Wavelength (A)

0.8

0.85

0.9

0.95

1

Nor

mal

ized

Flu

x

Fig. 4 Composite profile of Multiplet 7 of O I for HD42035 The vertical lines depict the laboratory wavelengthsof the O I lines.

unblended line, λ 4443.008 A to derive the zirconiumabundance. A few sharp lines have triangular profiles,they all can be identified as Fe II linesIn table 5, we have indicated as “broad” and some-times “asymmetric” the lines which show a broad shal-low component originating in HD 42035 B which cansometimes show an assymetry. These broad and shal-low lines are due to N I, O I, Mg II, Si II, Ti II and Fe II.From these identifications, we can infer that HD 42035B probably has an effective temperature which cannotdiffer much from that of HD 42035 S.A rough estimateof its projected rotational equatorial velocity has beenobtained by adjusting the broad component of the com-posite Mg II triplet profile at 4481 A with a model ofeffective temperature 10740 K, log g =3.80, solar metal-licity and yields ve sin i about 150 ± 25 km s−1.

5 Abundance determinations

5.1 Fundamental parameters determinations

For HD 67044, we have adopted the effective tempera-ture Teff = 10519 K and surface gravity log g = 3.72 de-rived by Huang et al. (2010) from fitting the Hγ profilesto prediction of model atmospheres. Indeed HD 67044does not have Stromgren’s photometry which precludesapplying Napiwotzky’s (1993) UVBYBETA procedureto derive its fundamental parameters. A spectrum syn-thesis of the Hγ profile was run to confirm these pa-rameters. For HD 42035, the effective temperature,Teff = 10740 K, and surface gravity, log g = 3.80, werealso taken from Huang et al. (2010). Applying Napi-wotzky’s procedure to the Stromgren’s photometry of

5

HD 42035 yields very similar fundamental parameters.The effective temperature obtained in this manner isprobably a complex mean of the individual effectivetemperatures of HD 42035 S and HD 42035 B as the

Stromgren’s photometry most likely measured the com-bination of the lights of both stars. The adopted effec-tive temperatures, surface gravities, projected equato-rial velocities and radial velocities of HD 67044 and HD

42035 S are collected in Table 2.

5.2 Model atmospheres and spectrum synthesiscalculations

Plane parallel model atmospheres assuming radiativeequilibrium and hydrostatic equilibrium were computedusing the ATLAS9 code (Kurucz 1992). The linelistwas built from Kurucz (1992) gfhyperall.dat and its re-vision gfall18sep15.dat 2 which includes hyperfine split-

ting levels. A grid of synthetic spectra was computedwith SYNSPEC48 (Hubeny & Lanz 1992) to model thelines of He I, C II, O I, Mg II, Al I and Al II, Si II, Ca II,Sc II, Ti II, Cr II, Mn II, Fe II, Sr II, Y II, Zr II, Ba II

and Hg II lines. Computations were iterated varyingthe unknown abundance until minimization of the chi-square between the observed and synthetic spectrumwas achieved. The microturbulent velocity was first as-sumed to be 1.5 kms−1 (in agreement with the run of

vmicr with Teff we established in Gebran et al. (2014)).The synthesis of the Fe II lines of various strengths how-ever imposed a lower vmicr = 0 km s−1 for HD 67044typical of an HgMn star. A null microturbulent veloc-

ity was also finally adopted for HD 42035 S after un-successful attempts to model the Fe II lines with highervelocities.

5.3 The derived abundances of HD 67044

We have used only unblended lines to derive the abun-dances. There are actually few unblended lines as theprojected equatorial velocity of HD 67044 broadens sig-nificantly the lines. For a given element, the final abun-

dance is a weighted mean of the abundances derived foreach transition. These final abundances and their esti-mated uncertainties for HD 67044 are collected in Table

2http://kurucz.harvard.edu/linelists/gfnew/gfall28sep15.dat

Table 2 Fundamental parameters

Star ID Teff log g v sin i Vrad

(km s−1) (km s−1)

HD 67044 10519 3.72 45.0 14.50

HD 42035 S 10740 3.80 3.7 53.00

3 (the determination of the uncertainties is discussed in

Royer et al. 2014). Table 3 contains for each analysedspecies the adopted laboratory wavelength, logarithm

of oscillator strength, its source, the logarithm of the

absolute abundance normalised to that of hydrogen (on

a scale where log(NH) = 12) for each transition, andthe final abundance and estimated uncertainty. In this

work, we adopted Asplund et al. (2009) abundances for

the Sun as a reference.

The iron abundance, which is found to be about solar

in HD 67044, has been derived mostly by using severalFe II lines of multiplets 37, 38 and 186 in the range

4500–4600A whose atomic parameters are critically as-

sessed in NIST3 (these are C+ and D quality lines).

These lines are widely spaced and the continuum isfairly easy to trace in this spectral region. Their syn-

thesis always yields consistent iron abundances from the

various transitions with very little dispersion. The iron

abundance is probably the most accurately determined

of the abundances derived here. The NLTE abundancecorrection for the λ 4471.48 A He I line is very small

as shown by Lemke (1989) for early A-type stars and

we have not corrected for it. We find that the following

species are underabundant: He, C, O, Si, Ca, Sc whileMg, V, Fe and Ni show mild enhancements (less than

5 times solar) and Ti, Cr, Mn, Sr, Y, Zr, Ba and Hg

show pronounced overabundances (larger than 5 times

solar)., the largest overabundance being for Hg. The

Sr-Y-Zr triad is inverted, yttrium beeing more abun-dant than strontium and zirconium. The general trend

is that the heaviest elements are the most overabun-

dant.

5.4 The provisional abundances for HD 42035 S

Assuming an effective temperature of 10740 K, log g =

3.80 and a solar composition, for HD 42035 S, we have

derived provisional abundances for HD 42035 S whichare collected in Table 4 The effective temperature of HD

42035 S is probably different from this mean value so

that the derived abundances are rough estimates only.

Furthermore, placing a continuum level in the compos-ite spectrum of HD 42035 turned out to be difficult

because of the presence of the rotationally broadened

lines and of the continuum of HD 42035 B. The provi-

sional abundances we derive here are therefore affected

by systematic errors due to (at least) the possibility ofan improper placement of the continuum (too low com-

pared to what it actually is). As a consequence, the

residual fluxes F

Fc

are likely to be too large, placing the

continuum higher would decrease these residual fluxes

3http://www.nist.gov

6

and therefore lead to higher abundances. We therefore

consider that the provisional abundances derived hereare lower limits. The actual abundances of HD 42035

S must be larger than these lower limits. To minimize

this effect we chose to synthesize sharp lines which were

as little as possible blended with the broad lines of HD42035 B. Realistic abundances will only be derived if

we manage to disentangle the spectrum of HD 42035 S

from that of HD 42035 B.

We find that the light elements up to Z=21, C, O, Mg,

Al, Si, S, Ca and Sc are all underabundant. The scan-dium deficiency is large (about 4 % of the solar scan-

dium abundance). The elements heavier than Z=21 are

overabundant except for Ti, Fe and Sr which are un-

derabundant. The zirconium overabundance has beenderived from only one unblended line and thus should

be taken with caution. The absence of detection of the

two strongest Y II lines at 3982.60 A and 5662.92 A

implies that yttrium must be solar or underabundant.

6 Conclusions

We find that HD 67044, hitherto classified a normalB8 star, displays underabundances of He, C, O, Si, Ca

and Sc, mild overabundances of Mg, V, Fe and Ni and

pronounced enhancements of Ti, Cr, Mn, Sr, Y, Zr, Ba

and Hg.. We therefore propose that HD 67044 actu-

ally is a new HgMn star and should be reclassified assuch. Current monitoring of HD 67044 suggests that

the Hg II line at 3983.93 A is probably variable. One

possible interpretation is that HD 67044 has one or sev-

eral spots of overabundant Hg over its surface. Moreobservations are planed to address this issue.

The high resolution spectrum of HD 42035 appears to

be a composite spectrum where redshifted very sharp

lines originating from HD 42035 S are overimposed onto

the broad shallow lines originating from HD 42035 B.The presence of a very slow rotator and a fairly fast ro-

tator inside the same system suggests that the semi-axis

of the orbit must be large. A FT analysis of the sharp

lines of HD 42035 S yields a very low projected equa-torial velocity (ve sin i = 3.7 km s−1) which makes this

star one of the very few late-B type slow rotators. The

identification of 713 very sharp lines reveals that most

of the lines are due to elements up to Nickel. Stron-

tium and Barium are also present. Assuming a similareffective temperature and surface gravity for HD 42035

S and HD 42035 B, we have derived provisional abun-

dances for HD 42035 S. Light elements up to Z=22 ap-

pear to be underabundant in HD 42035 S whereas heav-ier elements are overabundant with the exception of Fe

and Sr. These preliminary abundances are lower limits

of the actual abundances of HD 42035 S because we are

probably placing the continuum too low. A completefollow-up of this new spectroscopic binary will hope-

fully enable a proper disentangling of the spectra of HD

42035 S and HD 42035 B and help characterize fully the

nature of each of these components, in particular thenature and abundance pattern of HD 42035 S.

We thank the referee, Dr. Fiorella Castelli, for her

insightful comments which resulted into many improve-

ments. We also thank the OHP night assistants for

their helpful support during the three observing runs.

We acknowledge the use of the ELODIE archive atOHP.

7

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Sansonetti, C. J. & Reader, J. 2001, Physica Scripta, 63,219

Shenstone, A. G. 1961, Proceedings of the Royal Societyof London A: Mathematical, Physical and EngineeringSciences, 261, 153

Siegel, W., Migdalek, J., & Kim, Y.-K. 1998, Atomic Dataand Nuclear Data Tables, 68, 303

Theodosiou, C. E. 1989, Phys. Rev. A, 39, 4880Wiese, W. L., Fuhr, J. R., & Deters, T. M. 1996, Atomic

transition probabilities of carbon, nitrogen, and oxygen :a critical data compilation

This manuscript was prepared with the AAS LATEX macros v5.2.

8

Table 3 Elemental Abundances for HD67044. References are MA60 for Martin (1960), DR2006 for Drake

(2006), NS81 for Nussbaumer & Storey (1981), KZ91 for Butler, K. & Zeippen, C. J. (1991), W96 for

Wiese et al. (1996), HBGV91 for Hibbert et al. (1991), Si98 for Siegel et al. (1998), K79 for Kaufman & Hagan(1979), H99 for Hannaford (1999), Ma01 for Matheron et al. (2001), Sh61 for Shenstone (1961), LD89 for

Lawler & Dakin (1989), FMW for Fuhr et al. (1988), PTP for Pickering et al. (2002), SN14 for

Sansonetti & Nave (2014), NJ13 for Nave & Johansson (2013), T89 for Theodosiou (1989), RU98 for

Raassen & Uylings (1998), PBL95 for Pinnington et al. (1995), NBS for Miles & Wiese (1969), KO83 forKostyk & Orlova (1983), Bie11 for Biemont et al. (2011),L06 for Ljung et al. (2006), MCS75 for Meggers et al.

(1975), BL48 for Biermann & Lubeck (1948), Bal81 for Biemont et al. (1981), KL01 for Kling et al. (2001),

DSVD92 for Davidson et al. (1992), SR01 for Sansonetti & Reader (2001), Do03 for Dolk et al. (2003), NIST for

the online database (http://physics.nist.gov/PhysRefData/ASD/), and Kurucz

(http://kurucz.harvard.edu/linelists/gfhyperall/) for the gfhyperall.dat linelist.

Element λ (A) log gf Ref. log(X/H)⋆

He I 4471.470 -2.211 Ma60/DR2006 -1.17

He I 4471.474 -0.287 Ma60/DR2006 -1.17

He I 4471.474 -1.035 Ma60/DR2006 -1.17

He I 4471.485 -1.035 Ma60/DR2006 -1.17He I 4471.489 -0.558 Ma60/DR2006 -1.17

He I 4471.683 -0.910 Ma60/DR2006 -1.17

He I 5875.598 -1.516 Ma60/DR2006 -1.13

He I 5875.613 -0.339 Ma60/DR2006 -1.13He I 5875.615 0.409 Ma60/DR2006 -1.13

He I 5875.625 -0.339 Ma60/DR2006 -1.13

He I 5875.640 0.138 Ma60/DR2006 -1.13

He I 5875.966 -0.214 Ma60/DR2006 -1.15

[He

H] = −0.15± 0.15 dex

C II 4267.001 0.563 NS81 -4.06

C II 4267.261 0.716 NS81 -4.10C II 4267.261 -0.584 NS81 -4.10

[C

H] = −0.60± 0.15 dex

O I 5329.673 -2.063 KZ91/W96 -3.39O I 5330.726 -2.416 KZ91/W96 -3.37

O I 5330.741 -0.983 KZ91/W96 -3.37

O I 6155.961 -1.363 HBGV91 -3.41

O I 6155.971 -1.011 HBGV91 -3.41

O I 6155.989 -1.120 HBGV91 -3.41O I 6156.737 -1.487 HBGV91 -3.37

O I 6155.755 -0.898 HBGV91 -3.37

O I 6156.778 -0.694 HBGV91 -3.37

O I 6158.149 -1.841 HBGV91 -3.39O I 6158.172 -0.995 HBGV91 -3.39

O I 6158.187 -0.409 HBGV91 -3.39

[O

H] = −0.22± 0.20 dex

Mg II 4390.572 -0.523 Si98 -4.25

Mg II 4427.994 -1.208 Si98 -4.29

Mg II 4481.126 0.749 BL48 -4.27

Mg II 4481.150 -0.553 BL48 -4.27

Mg II 4481.325 0.594 BL48 -4.27

[Mg

H] = 0.15± 0.18 dex

Al II 4663.056 -0.244 K79 -5.56

Al I 3944.006 -0.635 H99 -5.60

9

Table 3—Continued

Element λ (A) log gf Ref. log(X/H)⋆

[Al

H] = −0.04± o.20 dex

Si II 4128.054 0.359 Ma01 -4.52

Si II 4130.894 0.552 Ma01 -4.56

Si II 4190.72 -0.351 Sh61 -4.54Si II 5041.024 0.029 Ma01 -4.56

Si II 5055.984 0.523 Ma01 -4.54

Si II 5056.317 -0.492 Ma01 -4.52

Si II 6347.11 0.149 Ma01 -4.54

Si II 6371.37 -0.082 Ma01 -4.56

[Si

H] = −0.086± 0.18 dex

Ca II 3933.663 0.135 NIST/T89 -6.02

Ca II 5019.971 -0.28 NIST/T89 -6.06

[Ca

H] = −0.40± 0.20 dex

Sc II 4246.822 0.242 LD89 -9.05

Sc II 4670.407 -0.580 LD89 -9.09Sc II 5031.021 -0.400 LD89 -9.07

Sc II 5526.813 -0.77 LD89 -9.07

[Sc

H] = −0.24± 0.18 dex

Ti II 4163.644 -0.128 PTP -5.97

Ti II 4287.873 -2.020 PTP -6.01

Ti II 4290.210 -0.848 PTP -5.99

Ti II 4294.090 -1.100 PTP -5.96

Ti II 4300.042 -0.442 PTP -5.97Ti II 4411.072 -0.6767 PTP -6.01

Ti II 4468.492 -0.620 FMW -5.99

Ti II 4549.622 -0.105 PTP -5.97

Ti II 4563.758 -0.96 Kurucz -5.99Ti II 5129.156 -1.239 KO83 -5.97

Ti II 5188.687 -1.220 PTP -6.00

Ti II 5336.780 -1.700 PTP -6.01

[T i

H] = 0.99± 0.20 dex

Cr II 4558.644 -0.660 SN14 -5.39

Cr II 4558.787 -2.460 SN14 -5.39

Cr II 5237.322 -1.160 SN14 -5.43

Cr II 5308.421 -1.810 SN14 -5.39Cr II 5313.581 -1.650 SN14 -5.41

Cr II 5502.086 -1.990 SN14 -5.43

[Cr

H] = 0.92± 0.18 dex

Mn II 4206.368 -1.54 KL01 -5.59

Mn II 4259.19 -1.44 KL01 -5.63

[Mn

H] = 1.060± 0.20 dex

Fe II 4233.162 -1.810 NJ13 -4.34

Fe II 4258.148 -3.500 NJ13 -4.30

Fe II 4273.326 -3.350 NJ13 -4.32

Fe II 4296.566 -2.900 NJ13 -4.30

10

Table 3—Continued

Element λ (A) log gf Ref. log(X/H)⋆

Fe II 4491.397 -2.640 NJ13 -4.34

Fe II 4508.280 -2.300 NJ13 -4.32

Fe II 4515.333 -2.360 NJ13/RU98 -4.34Fe II 4520.218 -2.600 NJ13/RU98 -4.32

Fe II 4522.628 -1.990 NJ13/RU98 -4.34

Fe II 4549.195 -1.770 NJ13/RU98 -4.30

Fe II 4549.466 -1.730 NJ13/RU98 -4.30Fe II 4555.888 -2.250 NJ13/RU98 -4.32

Fe II 4923.921 -1.210 NJ13 -4.34

Fe II 5275.997 -1.900 NJ13 -4.30

Fe II 5316.609 -1.780 NJ13/RU98 -4.32

Fe II 5506.199 0.860 NJ13 -4.30

[Fe

H] = 0.18± 0.18 dex

Sr II 4215.519 -0.173 PBL95 -7.67

[Sr

H] = 1.40± 0.25 dex

Y II 3982.592 -0.560 Bie11 -6.71

Y II 5662.922 0.340 Bie11 -6.75

[Y

H] = 3.05± 0.25 dex

Zr II 3991.127 -0.310 L06 -7.11

Zr II 3998.965 -0.520 L06 -7.09

Zr II 4442.992 -0.420 L06 -7.07Zr II 4457.431 -1.220 L06 -7.09

Zr II 4496.962 -0.890 L06 -7.07

Zr II 5112.270 -0.850 L06 -7.11

[Zr

H] = 2.30± 0.25 dex

Ba II 4934.077 -0.156 NBS -7.63

Ba II 6141.713 -0.032 DSVD92 -7.59

[Ba

H] = 2.18± 0.25 dex

Hg II 3983.931 -1.510 SR01/Do03 -7.21

[Hg

H] = 3.70± 0.25 dex

11

Table 4 Provisional Elemental Abundances for HD42035 S

Element λ (A) log gf Ref. log(X/H)⋆

C II 4267.001 0.563 NS81 -3.63

C II 4267.261 0.716 NS81 -3.63

C II 4267.261 -0.584 NIST -3.63

[C

H] = −0.15± 0.15 dex

O I 6155.961 -1.363 HBGV91 -3.47

O I 6155.971 -1.011 HBGV91 -3.47

O I 6155.989 -1.120 HBGV91 -3.47O I 6156.737 -1.487 HBGV91 -3.47

O I 6155.755 -0.898 HBGV91 -3.47

O I 6156.778 -0.694 HBGV91 -3.47

O I 6158.149 -1.841 HBGV91 -3.47

O I 6158.172 -0.995 HBGV91 -3.47O I 6158.187 -0.409 HBGV91 -3.47

[O

H] = −0.30± 0.20 dex

Mg II 4390.572 -0.530 Si98 -4.94Mg II 4427.994 -1.201 Si98 -4.94

Mg II 4481.126 0.730 BL48 -4.94

Mg II 4481.150 -0.570 BL48 -4.94

Mg II 4481.325 0.575 BL48 -4.94

[Mg

H] = −0.52± 0.18 dex

Al II 5593.27 +0.41 K79 -5.83

Al II 6243.40 +0.67 K79 -5.83

[Al

H] = −0.30± 0.20 dex

Si II 4128.054 0.306 Ma01 -5.05

Si II 4130.88 0.464 Ma01 -5.05

Si II 4190.72 -0.351 Sh61 -4.85Si II 5041.024 0.174 Ma01 -4.80

Si II 5055.984 0.441 Ma01 -4.85

Si II 5056.317 -0.535 Ma01 -4.75

Si II 6347.11 0.230 Ma01 -4.85Si II 6371.37 -0.080 Ma01 -4.85

[Si

H] = −0.43± 0.18 dex

S II 4162.665 0.830 Kurucz -4.97

[S

H] = −0.30± 0.20 dex

Ca II 3933.663 -0.135 NIST/T89 -5.94

Ca II 5019.971 -0.257 NIST/T89 -5.94

[Ca

H] = −0.30± 0.20 dex

Sc II 4246.86 0.242 LD89 -10.23

Sc II 4314.06 -0.10 LD89 -10.23

Sc II 4400.38 -0.51 LD89 -10.23Sc II 5031.021 -0.400 LD89 -10.23

[Sc

H] = −1.40± 0.18 dex

Ti II 4163.644 -0.130 PTP -7.20Ti II 4287.873 -1.790 PTP -7.20

Ti II 4290.210 -0.850 PTP -7.28

12

Table 4—Continued

Element λ (A) log gf Ref. log(X/H)⋆

Ti II 4300.042 -0.440 PTP -7.20Ti II 4411.072 -0.670 PTP -6.98

Ti II 4549.62 -0.470 PTP -7.20

Ti II 4563.77 -0.96 Kurucz -7.20

Ti II 5129.156 -1.400 KO83 -7.20

Ti II 5188.687 -1.050 PTP -7.28

[T i

H] = −0.21± 0.20 dex

V II 4005.706 -0.460 Kurucz -7.30

V II 4023.360 -0.880 Kurucz -7.30V II 4035.610 -0.960 Kurucz -7.30

[V

H] = 0.70± 0.20 dex

Cr II 4558.650 -0.660 SN14 -5.93Cr II 4558.78 -2.460 SN14 -5.93

Cr II 5237.329 -1.160 SN14 -6.02

Cr II 5308.440 -1.810 SN14 -6.02

Cr II 5502.067 -1.990 SN14 -6.02

[Cr

H] = 0.35± 0.18 dex

Mn II 4206.368 -1.566 KL01 -5.77

Mn II 4259.19 -1.589 KL01 -5.77

[Mn

H] = 0.85± 0.20 dex

Fe II 4233.172 -2.000 NJ13 -5.50

Fe II 4258.154 -3.400 NJ13 -4.90

Fe II 4273.326 -3.258 NJ13 -4.80Fe II 4296.570 -3.010 NJ13 -4.90

Fe II 4491.405 -2.690 NJ13 -5.32

Fe II 4508.281 -2.210 NJ13 -5.32

Fe II 4515.334 -2.490 NJ13/RU98 -5.20

Fe II 4520.221 -2.600 NJ13/RU98 -5.20Fe II 4522.628 -2.030 NJ13/RU98 -5.50

Fe II 4549.197 -1.870 NJ13/RU98 -4.50

Fe II 4549.467 -1.750 NJ13/RU98 -5.50

Fe II 4555.888 -2.290 NJ13/RU98 -5.20Fe II 4923.927 -1.320 NJ13 -5.32

Fe II 5276.002 -1.940 NJ13 -5.20

Fe II 5316.615 -1.850 NJ13/RU98 -5.20

Fe II 5506.195 0.950 NJ13 -5.02

[Fe

H] = −0.66± 0.18 dex

Ni II 5058.38 +0.85 Kurucz -4.75

Ni II 5059.17 +0.54 Kurucz -4.75

[Ni

H] = 1.00± 0.25 dex

Sr II 4077.709 0.148 PBL95 -9.53

Sr II 4215.520 -0.173 PBL95 -9.53

[Sr

H] = −0.46± 0.25 dex

Y II 5662.93 0.16 MCS75 -9.78

[Y

H] = 0.00± 0.25 dex

13

Table 4—Continued

Element λ (A) log gf Ref. log(X/H)⋆

Zr II 4443.008 -0.330 L06 -8.69

[Zr

H] = 0.70± 0.25 dex

Ba II 4554.029 +0.170 NBS -9.31

Ba II 4934.076 -0.156 NBS -9.31

Ba II 6496.897 -0.380 DSVD92 -9.31

[Ba

H] = 0.48± 0.25 dex

14

Table 5 Proposed line identifications for HD 42035 S

Corr. Lab. Ident. Elow log(gf) Rem.λ (A) λ (A) (cm−1)

3900.54 3900.550 Ti II 9118.260 -0.45

3902.95 3902.945 Fe I 12560.933 -0.47

3903.26 3903.268 V II 11908.270 -0.89

3903.74 3903.756 Fe II 60807.228 -1.49

3905.52 3905.525 Si I 15394.369 -1.093905.64 3905.644 Cr II 42986.619 -0.90

3906.03 3906.035 Fe II 44929.549 -1.83

3913.46 3913.468 Ti II 8997.710 -0.53

3914.50 3914.503 Fe II 13474.411 -4.053918.52 3918.528 Fe II 47674.718 -2.10

3918.95 3918.965 C II 131724.372 -0.51

3920.63 3920.635 Fe II 60625.451 -1.20

3921.99 3922.004 Fe II 72603.502 -1.06

3922.90 3922.908 Mg I 35051.263 -3.533927.92 3927.920 Fe I 888.132 -1.59

3930.30 3930.297 Fe I 704.007 -1.59

3930.304 Fe II 13673.186 -4.03

3932.00 3932.023 Ti II 9118.260 -1.783933.23 3933.245 Fe II 78690.849 -3.39

3933.34 3933.345 V II 47101.889 -2.69

3933.66 3933.663 Ca II 0.000 0.13

3935.95 3935.962 Fe II 44915.046 -1.86

3938.29 3938.290 Fe II 13474.411 -3.893938.97 3938.970 Fe II 47674.718 -1.85

3944.00 3944.006 Al I 0.000 -0.62

3945.20 3945.210 Fe II 13673.186 -4.25

3947.29 3947.295 O I 73768.202 -2.283947.48 3947.481 O I 73768.202 -2.43

3951.94 3951.930 Ni II 94705.927 -2.78

3951.965 V II 11908.270 -0.74

3960.89 3960.899 Fe II 58631.532 -1.42

3961.51 3961.520 Al I 112.061 -0.323968.46 3968.469 Ca II 0.000 -0.17

3979.51 3979.505 Cr II 45730.581 -0.73

4002.08 4002.083 Fe II 22409.852 -3.47

4002.53 4002.543 Fe II 48039.087 -1.714002.93 4002.936 V II 11514.760 -1.81

4003.28 4003.283 Cr II 52297.808 -0.60

4005.24 4005.242 Fe I 12560.933 -0.61

4005.70 4005.706 V II 14655.630 -0.46

4012.50 4012.496 Cr II 45669.369 -0.894015.47 4015.474 Ni II 32523.540 -2.42

4023.36 4023.388 V II 14556.090 -0.88

4024.54 4024.547 Fe II 36252.917 -2.48

15

Table 5—Continued

Corr. Lab. Ident. Elow log(gf) Rem.

λ (A) λ (A) (cm−1)

4025.12 4025.131 Ti II 4897.650 -1.98

4026.26 4026.201 He I 169086.766 -2.629

4026.26 4026.201 He I 169086.766 -1.4534026.26 4026.201 He I 169086.766 -0.705

4026.26 4026.201 He I 169086.843 -1.453

4026.26 4026.201 He I 169086.843 -0.976

4028.33 4028.343 Ti II 15257.430 -1.00

4028.77 4028.750 S II 128599.162 -0.124030.34 4030.358 Cr II 25033.700 -3.56

4030.358 Fe II 88723.398 -0.99

4030.72 4030.730 Mn I 0.000 -0.47

4031.45 4031.442 Fe II 38164.195 -3.114032.94 4032.935 Fe II 36252.917 -2.70

4035.61 4035.627 V II 14461.750 -0.96

4037.95 4037.972 Cr II 52321.010 -0.56

4044.00 4044.012 Fe II 44929.549 -2.41

4045.80 4045.812 Fe I 11976.238 0.284048.83 4048.830 Fe II 44915.046 -2.15

4049.09 4049.097 Cr II 52297.808 -0.86

4051.93 4051.930 Cr II 25033.700 -2.19

4053.82 4053.834 Ti II 15265.619 -1.214054.08 4054.076 Cr II 25046.759 -2.47

4057.46 4057.461 Fe II 58666.256 -1.55

4061.77 4061.782 Fe II 48039.087 -2.65

4063.59 4063.594 Fe I 12560.933 0.07

4067.03 4067.031 Ni II 32499.529 -1.294069.88 4069.883 Fe II 47674.718 -2.75

4070.64 4070.630 Fe II 60625.451 -3.01

4070.632 Fe II 62151.561 -2.98

4070.83 4070.840 Cr II 52321.010 -0.754071.04 4071.007 Ni II 32523.540 -3.47

4071.57 4071.564 V I 15572.030 -0.19

4071.73 4071.738 Fe I 12968.554 -0.02

4072.08 4072.097 Co II 25147.370 -4.72

4072.56 4072.561 Cr II 29951.880 -2.414072.70 4072.709 Si II 79338.550 -2.37

4075.44 4075.452 Si II 79355.019 -1.40

4075.93 4075.954 Fe II 20516.959 -3.38

4076.78 4076.780 Si II 79338.502 -1.674077.16 4077.15 Ti I 17423.855 -0.65

4077.71 4077.709 Sr II 0.000 0.17

4110.98 4110.990 Cr II 30307.439 -2.02

4111.003 Cr II 25033.700 -1.92

4111.85 4111.877 Fe II 48039.087 -2.16

16

Table 5—Continued

Corr. Lab. Ident. Elow log(gf) Rem.

λ (A) λ (A) (cm−1)

4113.23 4113.212 Cr II 25046.749 -2.27

4118.54 4118.545 Fe I 28819.952 0.29

4119.51 4119.524 Fe II 20516.959 -4.924120.85 4120.846 P II 103339.144 -2.87

4122.66 4122.668 Fe II 20830.582 -3.38

4124.77 4124.787 Fe II 20516.959 -4.20

4127.03 4127.057 Cr II 45730.581 -1.77

4128.06 4128.054 Si II 79338.502 0.32 Mult 24128.74 4128.748 Fe II 20830.582 -3.77

4130.88 4130.872 Si II 79355.019 -0.82 Mult 2

4130.894 Si II 79355.019 0.48 Mult 2

4132.05 4132.058 Fe II 12968.554 -0.654132.42 4132.419 Cr II 30307.439 -2.35

4142.23 4142.259 S II 127825.085 0.24

4143.42 4143.415 Fe I 24574.652 -0.20

4143.86 4143.868 Fe I 12560.933 -0.45

4145.07 4145.060 S II 127976.340 0.234145.78 4145.781 Cr II 42897.990 -1.16

4153.06 4153.068 S II 128233.187 0.39

4156.82 4156.799 Fe I 22838.320 -0.62

4160.63 4160.623 Fe II 22939.357 -5.044161.08 4161.075 Cr II 42986.619 -2.470

4161.52 4161.535 Ti II 8744.250 -2.360

4162.67 4162.665 S II 128599.162 0.83

4167.30 4167.299 Fe II 90300.626 -0.56

4171.88 4171.903 Cr II 25042.811 -2.384173.44 4173.461 Fe II 20850.582 -2.18

4177.68 4177.692 Fe II 20516.959 -3.75

4178.84 4178.862 Fe II 20830.582 -2.48

4179.42 4179.42 Cr II 30864.459 -1.774181.73 4181.732 Cr II 93574.441 -2.38

4187.03 4187.039 Fe I 19757.031 -0.55

4187.82 4187.805 V II 32299.271 -1.62

4190.72 4190.707 Si II 108820.600 0.20

4191.43 4191.430 Fe I 19912.494 -0.674192.02 4192.065 Ni II 32523.540 -3.06

4195.38 4195.365 Fe II 61041.746 -3.88

4196.17 4196.19 Fe II 90042.781 -3.04

4198.11 4198.134 Si II 108778.702 -0.304198.29 4198.304 Fe I 19350.891 -0.72

4199.09 4199.093 Fe II 37227.326 -3.99

4199.095 Fe I 24574.652 0.25

4199.48 4199.491 Fe II 89924.175 -0.23

4200.49 4200.521 Fe II 90067.346 -0.30

17

Table 5—Continued

Corr. Lab. Ident. Elow log(gf) Rem.

λ (A) λ (A) (cm−1)

4200.91 4200.898 Si II 101024.349 -0.67

4202.02 4202.029 Fe I 11976.238 -0.71

4202.52 4202.522 Fe II 54902.315 -2.334205.58 4205.595 Fe II 90386.527 -0.30

4210.35 4210.343 Fe I 20019.633 -0.87

4215.52 4215.519 Sr II 0.000 -0.14

4219.36 4219.360 Fe I 28819.952 0.12

4224.85 4224.860 Cr II 42986.619 -1.734226.72 4226.728 Ca I 0.000 0.24

4227.42 4227.427 Fe I 26874.547 0.23

4230.38 4230.375 Ni I 30619.440 -2.12

4232.47 4232.488 Ca I 39464.809 -2.604232.87 4232.849 Si II 97972.086 -1.00

4233.17 4233.172 Fe II 20830.582 -2.00

4233.62 4233.602 Fe I 20019.633 -0.60

4233.97 4233.977 V I 15688.870 -0.02

4234.15 4234.167 Nd II ? 1470.105 -0.994235.44 4235.421 Cr II 86782.041 -2.49

4235.92 4235.936 Fe I 19562.437 -0.34

4238.81 4238.791 Mn II 14781.190 -3.63

4242.36 4242.364 Cr II 31219.350 -0.594244.77 4244.779 Ni II 32523.540 -3.11

4246.82 4246.826 Sc II 2540.950 0.32 hfs 3 lines

4247.81 4247.805 Ti I 16106.075 -3.63

4250.10 4250.119 Fe I 19912.594 -0.41

4250.42 4250.437 Fe II 61974.931 -1.754250.79 4250.787 Fe I 12560.933 -2.81

4251.72 4251.717 Mn II 49882.153 -1.06

4252.61 4252.632 Cr II 31117.390 -2.02

4252.96 4252.962 Cr II 91955.392 -2.954252.963 Mn II 49889.858 -1.14

4254.34 4254.336 Cr I 0.000 -0.11

4254.51 4254.522 Cr II 47354.440 -0.97

4258.15 4258.154 Fe II 21812.055 -3.40

4258.33 4258.340 Fe II 21308.04 -4.134259.19 4259.191 Si II 97972.086 -1.30

4260.47 4260.474 Fe I 19350.891 -0.02

4261.92 4261.913 Cr II 31168.581 -1.53

4263.86 4263.869 Fe II 62049.023 -1.714267.00 4267.001 C II 145549.272 0.61

4267.25 4267.261 C II 145570.705 0.77

4269.26 4269.277 Cr II 31082.940 -2.17

4271.14 4271.153 Fe I 19757.031 -0.35

4271.77 4271.760 Fe I 11976.238 -0.16

18

Table 5—Continued

Corr. Lab. Ident. Elow log(gf) Rem.

λ (A) λ (A) (cm−1)

4273.32 4273.326 Fe II 21812.055 -3.26

4274.78 4274.797 Cr I 0.000 -0.23

4275.76 4275.779 Ti I 18825.781 -1.134278.15 4278.159 Fe II 21711.917 -3.82

4282.42 4282.403 Fe I 17550.180 -0.81

4284.18 4284.188 Cr II 31082.940 -1.86

4286.27 4286.280 Fe II 62171.614 -1.62

4287.87 4287.872 Ti II 8710.440 -2.024290.21 4290.219 Ti II 9395.710 -1.12

4294.09 4294,099 Ti II 8724.250 -1.11

4294.90 4294.91 Fe I 26351.038 -2.71

4296.56 4296.572 Fe II 21812.055 -3.014299.21 4299,206 Ti I 14106.633 -0.01

4300.04 4300.049 Ti II 9518.060 -0.77

4301.91 4301.914 Ti II 9363.620 -1.16

4303.17 4303.176 Fe II 21812.055 -2.49

4306.92 4306.916 Cr II 47372.533 -1.184307.89 4307.863 Ti II 9395.710 -1.29

4312.85 4312.864 Ti II 9518.060 -1.16

4314.06 4314.076 Sc II 4987.790 -0.10 5 hfs lines

4314.29 4314.310 Fe II 21581.638 -3.484314.97 4314.975 Ti II 9363.620 -1.13

4314.979 Fe II 38164.195 -3.10

4318.16 4318.188 Fe II 63559.489 -1.98

4319.40 4319.413 Fe II 61726.078 -2.12

4319.67 4319.680 Fe II 63272.974 -1.764320.34 4320.340 Ni II 113407.314 -2.72

4320.72 4320.725 Sc II 4883.570 -0.26

4320.93 4320.960 Ti II 9395.710 -1.97

4321.32 4321.309 Fe II 63465.106 -1.834324.97 4324.984 Sc II 4802.870 -0.44 2 hfs lines

4325.53 4325.540 Fe II 49100.978 -2.31

4325.523 Cr II 93276.860 -0.39

4325.75 4325.762 Fe I 12968.554 -0.01

4326.65 4326.639 Mn II 42537.180 -1.254337.93 4337.915 Fe II 8710.440 -1.13

4351.76 4351.769 Fe II 21812.055 -2.10

4354.33 4354.344 Fe II 61726.078 -1.39

4357.56 4357.584 Fe II 49100.978 -2.114361.24 4361.247 Fe II 49506.935 -2.11

4362.10 4362.099 Ni II 32499.529 -2.72

4362.95 4362.924 Cr II 45669.369 -1.89

4363.26 4363.255 Mn II 44899.820 -1.91

4367.65 4367.659 Ti II 20891.660 -1.27

19

Table 5—Continued

Corr. Lab. Ident. Elow log(gf) Rem.

λ (A) λ (A) (cm−1)

4368.24 4368.242 O I 76794.977 -2.03

4368.258 O I 76794.977 -2.25

4369.39 4369.411 Fe II 22409.852 -1.674383.54 4383.545 Fe I 11976.238 0.20

4384.09 4384.094 Fe II 50212.823 -2.28

4384.31 4384.319 Fe II 21430.359 -3.50

4384.65 4384.637 Mg II 80619.500 -0.79

4385.38 4385.387 Fe II 22409.852 -2.574386.83 4386.844 Ti II 20951.620 -1.26

4387.95 4387.930 He I 171134.897 -0.887

4390.57 4390.514 Mg II 80650.022 -1.49

4390.572 Mg II 80650.022 -0.534391.82 4391.791 Cr II 44307.091 -2.60

4391.820 S II 128233.197 -0.56

4394.05 4394.051 Ti II 9850.900 -1.59

4395.03 4395.033 Ti II 8744.250 -0.66

4395.80 4395.817 Fe II 90487.811 -1.204399.76 4399.772 Ti II 9975.920 -1.27

4400.38 4400.379 Sc II 4883.570 -0.51

4404.74 4404.75 Fe I 12560.933 -0.14

4407.67 4407.678 Ti II 9850.900 -2.474409.51 4409.516 Ti II 9930.690 -2.57

4411.06 4411.07 Ti II 24961.031 -1.06

4413.58 4413.601 Fe II 21581.638 -3.87

4415.12 4415.122 Fe I 12968.554 -0.62

4416.82 4416.830 Fe II 22409.852 -2.604417.71 4417.719 Ti II 9395.710 -1.47

4418.32 4418.330 Ti II 9975.920 -2.46

4418.94 4418.957 Fe II 64087.418 -1.84

4419.61 4419.604 Cr II 94365.189 -0.264427.99 4427.994 Mg II 80619.500 -1.21

4431.60 4431.605 Fe II 64040.884 -1.77

4433.99 4433.988 Mg II 80650.022 -0.91

4443.80 4443.794 Ti II 8710.440 -0.70

4444.29 4444.299 Fe II 50157.455 -3.704444.53 4444.539 Fe II 50157.455 -2.53

4446.22 4446.237 Fe II 48039.087 -2.44

4449.60 4449.616 Fe II 63948.792 -1.59

4450.47 4450.482 Ti II 8744.250 -1.454451.54 4451.551 Fe II 40506.935 -1.84

4455.26 4455.266 Fe II 50512.823 -2.14

4461.42 4461.439 Fe II 20830.582 -4.11

4461.70 4461.706 Fe II 50212.823 -2.05

4464.44 4464.450 Ti II 9363.620 -2.08

20

Table 5—Continued

Corr. Lab. Ident. Elow log(gf) Rem.

λ (A) λ (A) (cm−1)

4468.49 4468.507 Ti II 9118.260 -0.60

4471.48 4471.470 He I 169086.767 -2.212

4471.48 4471.474 He I 169086.767 -1.0364471.48 4471.474 He I 169086.767 -0.287

4471.48 4471.486 He I 169086.843 -1.035

4471.48 4471.489 He I 169086.843 -0.558

4472.92 4472.928 Fe II 22939.357 -3.43

4476.01 4476.019 Fe I 22946.815 -0.974475.995 Fe II 90901.125 -1.03

4478.64 4478.637 Mn II 53597.132 -0.95

4480.71 4480.688 Fe II 50212.823 -2.39

4481.12 4481.126 Mg II 71490.190 0.744481.150 Mg II 71490.190 -0.56

4481.34 4481.325 Mg II 71491.064 0.59

4487.48 4487.497 Fe II 62049.023 -2.14

4488.31 4488.331 Ti II 25192.791 -0.82

4489.17 4489.179 Ca II 68056.909 -0.614489.179 Ca II 68056.909 -0.61

4489.183 Ca II 22810.356 -2.97

4491.40 4491.405 Fe II 23031.299 -2.70

4493.52 4493.513 Ti II 8710.440 -2.734493.529 Fe II 63876.319 -1.43

4494.54 4494.563 Fe I 17726.988 -1.14

4501.26 4501.273 Ti II 8997.710 -0.75

4507.09 4507.102 Fe II 62689.878 -1.92

4508.27 4508.288 Fe II 23031.299 -2.214511.77 4511.775 Cr II 52297.808 -1.37

4512.02 4512.056 Fe II 61974.931 -2.18

4515.32 4515.339 Fe II 22939.357 -2.48

4515.59 4515.57 Cr II 67369.139 -1.114515.609 Fe II 50212.823 -1.11

4518.33 4518.327 Ti II 8710.440 -2.55

4520.21 4520.224 Fe II 22637.205 -2.60

4522.63 4522.634 Fe II 22939.357 -2.03 3 Eu II hfs lines

4524.98 4524.997 Fe II 86124.299 -3.434528.60 4528.614 Fe I 17550.180 -0.82

4529.50 4529.474 Ti II 12676.970 -2.03

4529.569 Fe II 44929.549 -3.19

4533.96 4533.969 Ti II 9975.920 -0.774534.16 4534.168 Fe II 23031.299 -3.47

4539.58 4539.595 Cr II 32603.400 -2.53

4541.06 4541.058 Fe II 61973.931 -2.48

4541.51 4541.524 Fe II 23031.299 -3.05

4549.21 4549.192 Fe II 47674.718 -1.97

21

Table 5—Continued

Corr. Lab. Ident. Elow log(gf) Rem.

λ (A) λ (A) (cm−1)

4549.47 4549.474 Fe II 22810.356 -1.75

4549.62 4549.617 Ti II 12774.689 -0.45

4552.40 4552.400 Cr II 93966.448 -4.094552.410 S II 121528.718 -0.10

4553.63 4553.623 Cr I 31008.995 -3.95

4554.03 4554.03 Ba II 0.000 0.02 15 hfs lines

4554.99 4554.988 Cr II 32836.680 -1.38

4555.88 4555.893 Fe II 22810.356 -2.294558.64 4558.650 Cr II 32854.311 -0.66

4559.06 4559.079 Fe I 35379.205 -3.67

4563.74 4563.761 Ti II 9850.900 -0.96

4565.72 4565.74 Cr II 32603.400 -2.114571.96 4571.968 Ti II 12676.970 -0.53

4576.34 4576.340 Fe II 22939.357 -3.04

4579.52 4579.527 Fe II 50212.823 -2.51

4580.05 4580.063 Fe II 20830.582 -3.73

4582.82 4582.835 Fe II 22939.357 -3.104583.82 4583.837 Fe II 22637.205 -2.02

4588.20 4588.199 Cr II 32836.680 -0.63

4589.93 4589.958 Ti II 9975.920 -1.79

4590.75 4590.736 Fe II 50187.813 -3.994591.00 4591.004 Fe II 63272.974 -2.25

4592.05 4592.049 Cr II 32854.949 -1.22

4593.60 4593.606 Fe II 62049.023 -2.41

4593.81 4593.827 Fe II 23317.632 -4.92

4596.00 4596.015 Fe II 50212.823 -1.844598.47 4598.494 Fe II 62945.040 -1.50

4616.12 4616.124 Cr I 7927.443 -1.19

4616.62 4616.629 Cr II 32844.760 -1.29

4618.81 4618.803 Cr II 32854.949 -1.114620.50 4620.521 Fe II 22810.356 3.28

4621.40 4621.418 Si II 101023.046 -0.54

4621.71 4621.696 Si II 101024.349 -1.68

4625.89 4625.893 Fe II 48039.087 -2.20

4628.76 4628.786 Fe II 63272.974 -1.744629.32 4629.339 Cr II 22637.205 -2.37

4631.87 4631.873 Fe II 63465.106 -1.87

4364.07 4364.070 Cr II 32844.760 -1.24

4635.30 4635.316 Fe II 48039.087 -1.654638.04 4638.050 Fe II 62171.614 -1.52

4640.80 4640.812 Fe II 62171.614 -1.88

4648.93 4648.944 Fe II 20830.582 -4.39

4656.97 4656.981 Fe II 23317.632 -3.63

4663.05 4663.046 Al II 85481.348 -0.28

22

Table 5—Continued

Corr. Lab. Ident. Elow log(gf) Rem.

λ (A) λ (A) (cm−1)

4663.70 4663.708 Fe II 23317.632 -4.27

4665.55 4665.548 Ni II 55299.649 -1.82

4666.75 4666.758 Fe II 22810.356 -3.334670.16 4670.182 Fe II 20830.585 -4.10

4673.28 4673.256 Si II 103556.025 -0.60 Broad

4673.526 Si II 103556.025 -0.60

4680.90 4680.904 Fe I 37162.745 -2.51

4702.98 4702.991 Mg I 35051.263 -0.674716.26 4716.271 S II 109831.595 -0.32

4730.38 4730.395 Mn II 43339.420 -2.15

4731.45 4731.453 Fe II 23317.632 -3.36

4739.74 4739.709 Mg II 93311.112 -0.82 Broad4755.73 4755.727 Mn II 43528.639 -1.24

4764.72 4764.728 Mn II 43537.180 -1.35

4771.73 4771.742 C I 60393.138 -2.12

4779.98 4779.985 Ti II 16515.860 -1.37

4805.09 4805.085 Ti II 16625.110 -1.104812.35 4812.337 Cr II 31168.581 -1.80

4815.56 4815.552 S II 110268.595 0.18

4820.80 4820.834 Fe II 831366.488 -0.69

4824.12 4824.127 Cr II 31219.350 -1.224826.88 4826.888 Mn I 31076.421 -1.42

4831.19 4831.202 Fe II 61041.746 -2.77 Broad

4833.20 4833.197 Fe II 21430.359 -4.78

4836.22 4836.229 Cr II 31117.390 -2.25

4848.25 4848.235 Cr II 31168.581 -1.144864.31 4864.326 Cr II 31117.390 -1.37

4871.30 4871.318 Fe I 23110.937 -0.41

4872.11 4872.138 Fe I 21244.836 -0.60

4873.46 4873.438 Ni I 29832.811 -0.474874.02 4874.014 Ti II 24961.031 -0.79

4876.41 4876.399 Cr II 31082.940 -1.46

4883.28 4883.287 Fe II 82853.660 -0.64

4884.600 4884.607 Cr II 31117.390 -2.08

4890.76 4890.765 Fe I 23192.497 -0.434891.48 4891.485 Cr II 31150.901 -3.04

4891.492 Fe I 22996.673 -0.14

4893.82 4893.820 Fe II 22810.356 -4.45

4901.60 4901.623 Cr II 52321.010 -0.834908.15 4908.151 Fe II 83308.193 -0.30

4911.19 4911.193 Ti II 25192.791 -0.34

4912.45 4912.462 Cr II 52297.808 -0.95

4913.29 4913.292 Fe II 82978.679 0.01

4918.98 4918.994 Fe I 23110.937 -0.37

23

Table 5—Continued

Corr. Lab. Ident. Elow log(gf) Rem.

λ (A) λ (A) (cm−1)

4920.49 4920.502 Fe I 22845.868 0.06

4921.931 HeI 171134.897 -0.443

4921.99 4922.006 Ni II 112719.745 -0.604923.92 4923.927 Fe II 23317.632 -1.32

4925.34 4925.343 S II 109560.686 -0.24

4948.06 4948.096 Fe II 83136.488 -0.32

4948.77 4948.793 Fe II 83459.671 -0.01

4951.57 4951.584 Fe II 83136.488 0.184952.64 4952.657 Fe II 83459.671 -0.65

4953.96 4953.987 Fe II 44929.549 -2.76

4957.27 4957.298 Fe I 22996.673 -0.34

4957.58 4957.596 Fe I 22650.414 0.134958.82 4958.822 Fe II 82713.536 -0.65

4967.89 4967.897 Fe I 33801.571 -0.53

4968.81 4968.832 Fe I 33946.932 -2.57

4977.02 4977.035 Fe II 83558.539 0.04

4984.48 4984.488 Fe II 83308.193 0.014990.50 4990.509 Fe II 83308.193 0.18

4991.43 4991.440 Fe II 82853.660 -0.57

4992.01 4992.024 Ni II 98822.511 0.99

4992.35 4992.358 Cr II 47354.440 -4.784999.17 4999.180 Fe II 82853.660 -0.48

5000.72 5000.743 Fe II 22409.852 -4.74

5001.48 5001.479 Ca II 60533.018 -0.52

5001.94 5001.959 Fe II 82853.660 0.90

5003.42 5003.414 Ni II 101144.633 0.705004.19 5004.195 Fe II 82853.660 0.50

5005.74 5005.742 Cr I 27728.811 -2.60

5006.11 5006.119 Fe I 22845.868 -0.62

5006.84 5006.841 Fe II 83713.536 -0.435007.44 5007.447 Fe II 83726.362 -0.36

5007.73 5007.739 Fe II 82978.679 -0.20

5008.98 5009.022 Fe II ? 83459.671 -0.41

5009.55 5009.567 S II 109831.595 -0.09

5014.05 5014.042 S II 113461.537 0.035014.062 Ni II 100332.090 -0.70

5014.067 Cr II 84604.840 -2.14

5014.95 5014.942 Fe I 31805.070 -0.25

5015.73 5015.755 Fe II 83459.671 -0.05 Broad asymetric5018.44 5018.440 Fe II 23317.632 -1.22

5021.56 5021.594 Fe II 82978.679 -0.30

5022.41 5022.420 Fe II 83459.671 -0.06

5022.78 5022.792 Fe II 82978.679 -0.02

5026.79 5026.806 Fe II 83136.488 -0.22

24

Table 5—Continued

Corr. Lab. Ident. Elow log(gf) Rem.

λ (A) λ (A) (cm−1)

5030.61 5030.630 Fe II 82978.679 0.40

5031.01 5031.010 Sc II 10944.560 -0.26

5031.88 5031.898 Fe II 83990.065 -0.785032.42 5032.434 S II 110268.595 0.28

5032.68 5032.712 Fe II 83812.317 0.11

5035.69 5035.708 Fe II 82978.679 0.61

5036.44 5036.427 Fe II 84359.799 -2.47

5041.02 5041.024 Si II 81191.341 0.295045.11 5045.114 Fe II 83136.488 -0.13

5047.64 5047.641 Fe II 83136.488 -0.07

5055.97 5055.984 Si II 81251.320 0.59

5056.31 5056.317 Si II 81251.320 -0.365056.70 5056.713 Cr II 69954.088 -1.68

5058.38 5058.376 Ni II 10357.203 0.85

5059.17 5059.20 Ni II 99132.784 0.54

5060.24 5060.257 Fe II 84266.557 -0.52

5061.70 5061.718 Fe II 83136.488 0.225065.07 5065.097 Fe II 84131.564 -0.45

5067.88 5067.893 Fe II 83308.193 -0.20

5070.89 5070.899 Fe II 83136.488 0.24

5072.00 5071.981 Fe II 90898.872 -1.625072.27 5072.281 Ti II 25192.791 -0.75

5074.05 5074.053 Fe II 54904.221 -1.97

5075.76 5075.764 Fe II 84326.910 0.28

5078.26 5078.296 Fe II 83990.065 -1.18

5082.23 5082.230 Fe II 83990.065 -0.105086.30 5086.306 Fe II 83990.065 -0.48

5087.30 5087.303 Fe II 83713.536 -0.50

5089.22 5089.214 Fe II 83308.193 -0.03

5093.56 5093.576 Fe II 83713.536 0.11 triangular5097.27 5097.271 Fe II 83713.536 0.31

5100.71 5100.127 Fe II 83726.362 0.70

5106.10 5106.097 Fe II 83812.317 -0.95

5106.109 Fe II 83308.193 -0.28

5117.03 5117.034 Fe II 84131.564 -0.135127.86 5127.866 Fe II 44929.549 -2.53

5129.14 5129.152 Ti II 15257.430 -1.39

5132.66 5132.669 Fe II 22637.205 -4.18

5139.46 5139.462 Fe I 23711.453 -0.575143.88 5143.880 Fe II 84266.557 0.10

5144.34 5144.355 Fe II 84424.372 0.18

5145.78 5145.772 Fe II 83990.065 -0.40

5146.10 5146.127 Fe II 22810.356 -3.91

5148.94 5148.907 Fe II 83990.065 -0.40

25

Table 5—Continued

Corr. Lab. Ident. Elow log(gf) Rem.

λ (A) λ (A) (cm−1)

5149.46 5149.465 Fe II 84266.557 0.40

5150.47 5150.489 Fe II 84266.557 -0.12

5151.27 5151.247 Cr II 70316.899 -3.215160.84 5160.839 Fe II 44915.046 -2.64 almost triangular

5163.58 5163.544 Fe II 84685.198 -1.90

5165.69 5165.633 N I 94770.879 -2.18 broad Fe II 5165.649 ?

5165.709 N I 94793.489 -3.35 Fe II 5165.751 ?

5166.55 5166.555 Fe II 84326.910 -0.03 triangular5167.33 5167.321 Mg I 21850.405 -1.03

5169.03 5169.033 Fe II 23317.632 -0.87

5170.78 5170.777 Fe II 84326.910 -0.36

5180.30 5180.314 Fe II 83812.317 0.045185.53 5185.520 Si II 103556.025 -0.27 broad

5185.555 Si II 103556.156 -0.39

5185.88 5185.913 Ti II 15265.639 -1.35

5186.85 5186.873 Fe II 84424.372 -0.30

5188.67 5188.680 Ti II 12758.110 -1.215191.43 5191.428 Cr II 30307.439 -3.36

5192.35 5192.344 Fe I 24180.861 -0.42

5193.72 5193.682 Fe II 93987.462 -3.30

5194.38 5194.384 Fe II 179893.560 -3.215194.89 5194.892 Fe II 84424.372 -0.15

5197.56 5197.577 Fe II 26055.422 -2.10

5199.11 5199.122 Fe II 83713.536 0.10

5200.78 5200.804 Fe II 83812.317 -0.37

5201.43 5201.468 Cr II 69954.088 -1.655203.63 5203.638 Fe II 83812.317 -0.05

5210.53 5210.539 Sc I 20236.860 0.43

5213.98 5213.960 Fe II 84527.779 -0.22

5215.34 5215.349 Fe II 83713.536 -0.015215.81 5215.844 Fe II 83726.362 -0.23

5216.85 5216.854 Fe II 84710.686 0.39

5216.863 Fe II 84527.779 0.61

5218.85 5218.842 Fe II 83726.362 -0.21

5222.36 5222.361 Fe II 84844.832 -0.335223.24 5223.260 Fe II 83812.317 -0.41

5223.80 5223.800 Fe II 83713.536 -0.59

5224.40 5224.411 Fe II 83990.065 -0.57

5225.34 5225.306 Cr II 86691.551 -0.665226.00 5225.968 Fe II 83812.317 -0.41

5226.54 5226.543 Ti II 12628.731 -1.30

5227.48 5227.481 Fe II 84296.829 0.80

5228.61 5228.648 Cr II 86078.899 -4.01

5228.68 5228.695 Fe II 93487.649 -3.70

26

Table 5—Continued

Corr. Lab. Ident. Elow log(gf) Rem.

λ (A) λ (A) (cm−1)

5232.49 5232.496 Cr II 32836.680 -2.09

5232.77 5232.787 Fe II 83726.362 -0.06

5232.94 5232.940 Fe II 23711.453 -0.195234.29 5234.271 V II 18269.490 -4.42

5234.62 5234.625 Fe II 25981.630 -2.05

5237.32 5237.329 Cr II 32854.311 -1.16

5237.329 Cr II 86782.041 -0.58

5239.80 5239.813 FeII 84326.910 -0.465245.45 5245.455 Fe II 84326.910 -0.51

5246.77 5246.768 Cr II 29951.880 -2.45

5247.95 5247.952 Fe II 84938.177 0.63

5249.39 5249.437 Cr II 30307.439 -2.435251.23 5251.233 Fe II 84844.832 0.51

5253.65 5253.641 Fe II 84296.829 -0.09

5254.91 5254.929 Fe II 26055.422 -3.23

5256.92 5256.938 Fe II 23317.632 -4.25

5257.12 5257.122 Fe II 84685.198 0.035260.24 5260.259 Fe II 84035.139 1.07

5262.31 5262.317 Fe II 85048.600 -0.36

5264.18 5264.177 Fe II 84710.686 0.36

5264.79 5264.812 Fe II 26055.422 -3.195272.39 5272.397 Fe II 48039.087 -2.03

5274.96 5274.964 Cr II 32836.680 -1.29

5275.98 5276.002 Fe II 25805.329 -1.94

5278.91 5278.938 Fe II 47674.718 -2.41

5279.87 5279.876 Cr II 32854.311 -2.105280.05 5280.054 Cr II 32854.949 -2.01

5284.09 5284.109 Fe II 23317.632 -3.19

5291.65 5291.666 Fe II 84527.779 0.58

5298.85 5298.860 Fe II 84844.832 -1.135302.38 5302.402 Mn II 79569.268 0.23

5303.40 5303.395 Fe II 66012.752 -1.61

5305.85 5305.853 Cr II 30864.459 -2.36

5306.17 5306.180 Fe II 84870.863 0.22

5308.41 5308.408 Cr II 32836.680 -1.815310.68 5310.687 Cr II 32844.760 -2.28

5313.57 5313.563 Cr II 32854.949 -1.65

5315.07 5315.086 Fe II 85048.600 -0.38

5315.55 5315.563 Fe II 66377.284 -1.465316.21 5316.225 Fe II 84035.139 0.34

5316.77 5316.784 Fe II 25981.630 -2.91

5318.06 5318.057 Fe II 84527.779 -0.14

5318.74 5318.750 Fe II 84035.139 -0.57

5322.23 5322.234 Fe II 84326.910 -0.52

27

Table 5—Continued

Corr. Lab. Ident. Elow log(gf) Rem.

λ (A) λ (A) (cm−1)

5324.18 5324.179 Fe I 25899.986 -0.24

5325.55 5325.553 Fe II 25981.630 -2.60

5329.12 5329.096 O I 86625.757 -2.08 triplet5329.70 5329.690 O I 86627.777 -1.41

5330.76 5330.741 O I 86631.453 -1.12

5334.86 5334.869 Cr II 32844.760 -1.56

5336.78 5336.771 Ti II 12758.110 -1.70 broad

5337.74 5337.732 Fe II 26055.422 -3.895339.59 5339.585 Fe II 84296.829 0.54

5347.19 5347.190 Fe II 85172.810 -0.28

5362.86 5362.869 Fe II 25805.329 -2.74

5366.20 5366.207 Fe II 84710.686 -0.275370.31 5370.309 Fe II 84710.686 -0.82

5375.83 5375.827 Fe II 85048.600 -0.75

5375.847 Fe II 84296.829 -0.29

5383.35 5383.369 Fe I 34782.420 0.50

5387.04 5387.063 Fe II 84863.353 0.525393.83 5393.847 Fe II 84296.829 -0.30

5395.84 5395.857 Fe II 85495.303 0.36

5401.60 5401.521 Mg II 93799.630 -0.45 triplet broad

5401.556 Mg II 93799.750 -1.885401.556 Mg II 93799.750 -0.34

5402.05 5402.059 Fe II 85184.734 0.50

5404.14 5404.117 Fe I 34782.420 0.54

5404.151 Fe I 35767.561 0.52

5405.07 5405.099 Fe II 85184.734 -1.015405.71 5405.663 Fe II ? 84870.863 -0.44

5407.62 5407.604 Cr II 30864.459 -2.09

5408.80 5408.811 Fe II 48039.087 -2.39

5414.05 5414.073 Fe II 25981.630 -3.795414.85 5414.862 Cr II 55023.098 -1.78

5415.19 5415.199 Fe I 35379.205 0.50

5420.88 5420.922 Cr II 30307.439 -2.36

5424.05 5424.068 Fe I 34843.954 0.52

5425.24 5425.257 Fe II 25805.329 -3.365427.80 5427.826 Fe II 54232.193 -1.66

5428.66 5428.655 S II 109560.686 -0.01

5429.96 5429.988 Fe II 85462.859 0.46

5432.95 5432.967 Fe II 26352.767 -3.635435.77 5435.775 O I 86627.777 -1.66

5436.86 5436.862 O I 86631.453 -1.51

5436.868 Cr II 86980.102 -0.47

5442.35 5442.351 Fe II 85048.600 -0.30

5444.40 5444.387 Fe II 85495.303 -0.18

28

Table 5—Continued

Corr. Lab. Ident. Elow log(gf) Rem.

λ (A) λ (A) (cm−1)

5445.79 5445.807 Fe II 85048.600 -0.11

5450.07 5450.099 Fe II 85679.698 -0.53

5453.83 5453.855 S II 110268.595 0.565455.42 5455.454 Fe I 34843.954 0.30

5455.879 Cr II 33618.941 -3.00

5455.90 5455.932 Fe II 84527.779 -0.52

5457.73 5457.730 Fe II 85728.806 -0.17

5465.93 5465.931 Fe II 85679.698 0.525466.40 5466.461 Si II ? 101023.046 -0.20

5466.89 5466.849 Si II 101024.349 -1.34

5466.894 Si II 101024.349 -0.04

5473.59 5473.590 Fe II 85172.810 -0.795473.614 S II 109560.686 -0.12

5475.81 5475.829 Fe II 84685.198 -0.18

5478.36 5478.365 Cr II 33694.151 -1.91

5479.40 5479.401 Fe II 85172.810 -0.41 triangular

5482.30 5482.308 Fe II 85184.734 0.435487.62 5487.619 Fe II 85462.859 0.36

5492.08 5492.079 Fe II 85679.698 -0.18

5492.39 5492.399 Fe II 84685.198 -0.06

5493.82 5493.833 Fe II 84685.198 0.215502.08 5502.067 Cr II 33618.941 -1.99

5502.67 5502.671 Fe II 85184.734 -0.14

5503.21 5503.211 Fe II 84685.198 -0.09

5503.212 Cr II 33417.991 -2.31

5506.18 5506.195 Fe II 84863.353 0.955507.05 5507.072 Fe II 84870.863 -0.32

5508.61 5508.606 Cr II 33521.110 -2.11

5510.75 5510.779 Fe II 85184.734 0.00

5525.12 5525.125 Fe II 26352.767 -4.61 triangular5528.40 5528.405 Mg I 35051.263 -0.62

5529.06 5529.053 Fe II 84870.863 -0.25

5529.93 5529.932 Fe II 54273.640 -1.87

5532.08 5532.088 Fe II 84870.863 -0.33

5534.82 5534.847 Fe II 26170.181 -2.935544.76 5544.763 Fe II 84863.353 0.12

5549.00 5549.001 Fe II 84870.863 -0.23

5554.93 5554.914 Fe II 85679.698 -0.64

5567.84 5567.842 Fe II 54283.218 -1.895577.94 5577.915 Fe II 85462.859 -0.14

5586.77 5586.756 Fe I 27166.817 -0.21

5587.08 5587.114 Fe II 54275.638 -2.18

5588.21 5588.220 Fe II 85462.859 0.09

5593.27 5593.300 Al II 106920.564 0.41

29

Table 5—Continued

Corr. Lab. Ident. Elow log(gf) Rem.

λ (A) λ (A) (cm−1)

5606.14 5606.151 S II 110766.562 0.16

5615.61 5615.644 Fe I 26874.547 -0.14

5627.47 5627.458 Cr II 87858.560 0.215640.32 5640.346 S II 110508.706 0.15

5643.86 5643.880 Fe II 61726.078 -1.46

5645.38 5645.392 Fe II 85184.734 0.08

5648.90 5648.904 Fe II 85184.734 -0.24

5657.91 5657.935 Fe II 27620.411 -4.105658.18 5658.111 Ni II 53037.932 -2.15

5658.79 5658.820 Fe II 85184.734 -0.72

5659.98 5660.001 S II 110313.403 -0.07

5691.00 5690.994 Fe II 86124.299 -0.205716.50 5716.59 Fe II 62689.878 -2.26 broad

5726.55 5726.557 Fe II 86416.331 -0.02

5747.87 5747.884 Fe II 44929.549 -2.91

5780.13 5780.128 Fe II 86124.299 0.32

5780.35 5780.336 Fe II 86416.331 -0.375783.61 5783.630 Fe II 86416.331 0.21

5784.43 5784.448 Fe II 86599.737 0.06

5813.67 5813.677 Fe II 44929.549 -2.75

5835.48 5835.492 Fe II 47674.718 -2.37 triangular5854.19 5854.192 Fe II 86599.737 -0.19

5875.10 5875.097 Fe II 87572.430 -2.36

5875.614 HeI 169086.766 -0.339

5875.615 HeI 169086.766 -0.409

5875.625 HeI 169086.843 -0.3395875.640 HeI 169086.843 0.138

5957.56 5957.559 Si II 81191.341 -0.30

5978.93 5978.930 Si II 81251.320 0.00

5990.97 5990.980 C I 69710.660 -3.585991.36 5991.376 Fe II 25428.783 -3.56

6071.38 6071.426 Fe II 86416.331 -0.19

6084.09 6084.111 Fe II 25805.329 -3.81

6103.49 6103.496 Fe II 50142.788 -2.17 triangular

6113.31 6113.322 Fe II 25981.630 -4.166143.04 6143.026 Fe II 60956.779 -3.82

6147.74 6147.741 Fe II 31364.440 -2.72

6149.25 6149.258 Fe II 31368.450 -2.72

6155.98 6155.961 O I 86625.757 -1.40 3 lines6156.78 6156.778 O I 86627.777 -0.73 3 lines

6158.18 6158.187 O I 86631.453 -0.44 3 lines

6175.13 6175.146 Fe II 50187.813 -1.98

6179.39 6179.384 Fe II 44915.046 -2.60

6239.79 6231.750 Al II 105441.498 0.40

30

Table 5—Continued

Corr. Lab. Ident. Elow log(gf) Rem.λ (A) λ (A) (cm−1)

6238.39 6238.392 Fe II 31364.440 -2.63

6239.62 6239.614 Si II 103556.025 0.19 3 lines

6239.93 6239.953 Fe II 31368.450 -3.44

6243.40 6243.367 Al II 105470.928 0.676247.55 6247.557 Fe II 31387.949 -2.33

6347.09 6347.109 Si II 65500.472 0.30 broad

6371.35 6371.371 Si II 65500.472 0.00 broad

6402.23 6402.246 Na I 134041.838 0.36

6416.92 6416.919 Fe II 31387.949 -2.74